assembly of massive elliptical galaxies
DESCRIPTION
Assembly of Massive Elliptical Galaxies. Mike Boylan-Kolchin UC Berkeley Mon. Not. Roy. Astron. Soc. 2005, 2006 astro-ph/0502495, 0601400. Massive Galaxies Over Cosmic Time 2. Eliot Quataert. Chung-Pei Ma. How important are gas-poor mergers for building massive elliptical galaxies?. - PowerPoint PPT PresentationTRANSCRIPT
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Assembly of Massive Elliptical Galaxies
Mike Boylan-KolchinUC Berkeley
Mon. Not. Roy. Astron. Soc. 2005, 2006astro-ph/0502495, 0601400
Massive Galaxies Over Cosmic Time 2
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Eliot Quataert
Chung-Pei Ma
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How important are gas-poor mergers for building massive elliptical
galaxies?– Expected in current galaxy formation models embedded in LCDM simulations
– Help explain dichotomy between bright and faint ellipticals
– Have been observed– Tension with evolution of galaxy luminosity functions?
– Consistency with tight observed scaling relations?
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Merger Simulations
• Model elliptical galaxy as Hernquist stellar bulge + NFW dark matter halo w/ and w/o adiabatic contraction) - no black holes, no gas
important: E0
• Simulate mass ratios of 1:1, 1:3
• Use distribution of orbits seen in cosmological dark matter simulations
• over 106 particles per simulation; run using GADGET
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Fundamental Plane
MBK, Ma, & Quataert (MNRAS, 2006)
Initial Condition
Virial Theorem:R-2 Mdyn
R-2 (Mdyn/L) L
Virial PlaneRee
2/Ie
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K-band FP:Re1.53±0.08 Ie-0.79±0.03
(Pahre et al. 1998)
Mdyn/LRe0.21
Tilt due to increasing dark matter fraction in with increasing Re
Fundamental Plane
MBK, Ma, & Quataert (MNRAS, 2006)
K-band FPRe1.53Ie-0.79
See also Capelato et al. 1995, Nipoti et al. 2003, Robertson et al. 2006
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M- and Re-M
relations
MBK, Ma, & Quataert (MNRAS, 2006)
Angular momentum
Full elliptical galaxy population: L4ReL0.6-0.7
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Brightest Cluster Galaxies• Clusters form at intersections of filaments natural preferred direction for merging
If BCGs are assembled by dissipationless mergers during cluster formation, orbits should be preferentially radial.
This radial merging will preserve the fundamental plane but lead to deviations in M and R M
:
> 4, > 0.6
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Normal Ellipticals
Oegerle & Hoessel (1991)
Very Massive Ellipticals & BCGs
Fundamental Plane
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Oegerle & Hoessel (1991)
Normal Ellipticals
Very Massive Ellipticals & BCGsFaber-Jackson
relation
-Mr
log()
Velocity dispersion roughly constant
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Desroches et al. 2006
“Normal” ellipticals
BCGs
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Desroches et al. 2006
R L0.7Non-BCGs
BCGs
BCGs+cDenvelope
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What About Black Holes?
• Dry assembly of BCGs / massive ellipticals:BH growth comes from mergers
Dry merger predictions for BCGs: Black hole mass traces galaxy stellar mass: MBHM
Different M- relation: M with >4
MBH- relation changes to >4
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L- correlation
Are black hole masses constant over ~0.6 dex in luminosity?
(see also Lauer et al. 2006, Bernardi et al. 2006)
MBH=5x109 Msun vs.MBH=1.5x1010 Msun for most massive BCGs
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Conclusions• The fundamental plane is preserved by dry merging
under a variety of orbital configurations and mass
ratios
• The FP projections do show dependence on merger
orbit, a result of dynamical friction energy loss
• Radial merging along filaments is a well-motivated
mechanism for producing BCGs; should lead to BCGs
following different FP projections from normal
ellipticals (now observed)
• Change in L- relation for massive galaxies means
using standard black hole mass predictor (MBH 4)
may underestimate black hole masses: BCGs could
host black holes of >1010 Msun
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Fundamental Plane Projections
scaling relations depend on energy and angular momentum of orbit
MBK, Ma, & Quataert (MNRAS, 2006)
Angular momentum
observed: M4
ReL0.6-0.7
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Predictions
• Dry mergers will preserve the fundamental plane
• If the mergers are on typical orbits (significant angular momentum), they will also preserve projections of the FP
• More radial mergers will lead to deviations in projections of the FP
Q: when (if ever) are low angular momentum mergers expected?
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B. Moore
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Fundamental Plane
R vs. L
Bernardi et al. 2006; also Lauer et al. 2006
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Deviations also seen for other massive ellipticals (Desroches, Quataert, Ma, and West 2006)
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Constraints on Galaxy Assembly
fundamental plane connects ellipticals’ half-light radii (Re), luminosities (L), and velocity dispersions (): (Djorgovski & Davis 1987, Dressler et al. 1987)
Re1.53±0.08 Ie-0.79±0.03 Re -3 L3/2 Pahre et al. 1998 (K-band)
virial theorem connects R, , and M
R -2 M R -2 (M/L) L require (M/L) L1/2 -1 or (tilt)
Locations in : L 4 (Faber-Jackson), R L0.7
contain more information than plane itself
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Future Work• Reproducing scaling relations is only one piece of the puzzle: need to understand if dry merging works in other ways too
• Need to embed merger simulations into cosmological environment: multiple mergers, realistic merging sequence
• Make predictions for black hole mass function and its evolution - implications for galaxy formation at higher redshifts?
• Observations: measure more black hole masses in BIG galaxies (using adaptive optics) to get better statistics
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Example: Virgo Cluster / M87
• Virgo / M87
– M6 x 1011 Msun
M87 340 km s-1
– MBH = 3.0 x 109 Msun
• Massive clusters:
– M, BCG1-3 x 1012 Msun (or more?)
– maximum 400 km s-1 – gives:
•MBH = 5.8 x 109 Msun (using MBH-)
•MBH = 2 x 1010 Msun (using MBH-M)
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SDSS: Bernardi et al. 2006
Projections:
L 4 (Faber-Jackson)
R L0.7
Projections carry more information than plane itself
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Solid Line:Virial theoremprediction
Fundamental Plane
MBK, Ma, & Quataert (MNRAS, 2006)
Initial Condition